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Astron. Astrophys. 328, 361-370


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Resonant Alfvén waves in coronal arcades
driven by footpoint motions

M.S. Ruderman1,4, M. Goossens2, J.L. Ballester3, and R. Oliver3

1Institute for Problems in Mechanics, Russian Academy of Sciences, 117526 Moscow, Russia
2Centre for Plasma Astrophysics, K.U. Leuven, Celestijnenlaan 200 B, B-3001 Heverlee, Belgium
3Departament de Física, Universitat de les Illes Balears, E-07071 Palma de Mallorca, Spain
4Present address: School of Mathematical and Computational Sciences, University of St Andrews, North Hough, St Andrews,
Fife KY16 9SS Scotland, UK

Received 12 June 1997 / Accepted 21 July 1997

Abstract

X-ray spectroscopy performed from different astronomical spacecrafts has shown that the solar corona is structured by magnetic fields having the shape of loops and arcades. These structures are formed by stretching and reconnection of magnetic fields, and remain stable from days to weeks. Also, sporadic or periodic brightenings of such structures have been detected in UV and soft X-ray observations, suggesting the existence of propagating waves and plasma heating within them. In this paper, a mechanism for the deposition of Alfvén wave energy and heating of coronal arcades via resonant absorption is investigated. An analytical solution to the linear viscous, resistive MHD equations that describes the steady state of resonant shear Alfvén oscillations in coronal arcades driven by toroidal footpoint motions is obtained. General expressions for the total amount of dissipated wave energy and for its spatial distribution within the resonant magnetic surface is derived.

Key words: MHD - wave - Sun: corona; oscillations

Send offprint requests to: M. Ruderman


© European Southern Observatory (ESO) 1997

Online publication: October 30, 1997
Last change: March 24, 1998
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